Detection of propadiene (CH 2 CCH 2), propene (C 3 H 6) and non-detection of propane (C 3 H 8) in Jupiter's northern polar stratosphere

We report the first detection of stratospheric propadiene (CH 2 CCH 2) and propene (C 3 H 6) at Jupiter's mid-to-high northern latitudes using IRTF-TEXES measurements recorded on March 5-6, 2025. Using radiative transfer software to quantitatively test for the presence of propadiene and propene, we report a > 12- sigma detection of propadiene and a > 17- sigma detection of propene inside Jupiter's northern auroral region (henceforth 'NAR'), where the species are most concentrated. For example, at 62 N inside Jupiter's NAR, we derive a 1-mbar propadiene abundance of 2.0 plus or minus 0.2 ppbv, which is 40 plus or minus 3 higher than abundances predicted by the Moses & Poppe (2017) photochemical model (henceforth 'MP17'), and significantly higher than the 1.2-ppbv upper limit abundance derived at 42 N (the lowest latitude sampled by the observations). Similarly, we derive a 1-mbar propene abundance of 8.1 plus or minus 0.5 ppbv at 62 N inside Jupiter's NAR, which is 28 plus or minus 2 higher than the MP17 predicted abundance and higher than the 6-ppbv 1-mbar upper limit abundance derived at 42 N. The fact that propadiene and propene are most enriched inside Jupiter's NAR strongly suggests that perturbations to the chemistry by auroral-related heating and exogenous ions/electrons are responsible for their significant enrichment. Spectral features of propane (C 3 H 8) were not detected at any of the locations sampled by the data: 3- sigma upper limits of 10 ppbv were derived at the 10-mbar level at 62 N inside Jupiter's NAR. The non-detection of propane could, in part, be explained by the vertical sensitivity of its spectral features to deeper pressures, where there is negligible auroral-related heating. The results of this work advocate for development of ion-neutral chemistry models of Jupiter's polar stratosphere.